scholarly journals HST/WFC3 grism observations ofz∼ 1 clusters: the cluster versus field stellar mass–size relation and evidence for size growth of quiescent galaxies from minor mergers

2018 ◽  
Vol 484 (1) ◽  
pp. 595-617 ◽  
Author(s):  
J Matharu ◽  
A Muzzin ◽  
G B Brammer ◽  
R F J van der Burg ◽  
M W Auger ◽  
...  
Keyword(s):  
Stellar Mass ◽  
Size Growth ◽  
Mass Size ◽  
Minor Mergers ◽  
Size Relation

scholarly journals HST/WFC3 grism observations of z ∼ 1 clusters: evidence for evolution in the mass–size relation of quiescent galaxies from post-starburst galaxies

2020 ◽  
Vol 493 (4) ◽  
pp. 6011-6032 ◽  
Author(s):  
J Matharu ◽  
A Muzzin ◽  
G B Brammer ◽  
R F J van der Burg ◽  
M W Auger ◽  
...  
Keyword(s):  
Rapid Change ◽  
Driving Mechanism ◽  
Cluster Galaxies ◽  
Star Forming ◽  
Large Size ◽  
The Galaxy ◽  
Size Growth ◽  
Mass Size ◽  
Minor Mergers ◽  
Size Relation

ABSTRACT Minor mergers have been proposed as the driving mechanism for the size growth of quiescent galaxies with decreasing redshift. The process whereby large star-forming galaxies quench and join the quiescent population at the large size end has also been suggested as an explanation for this size growth. Given the clear association of quenching with clusters, we explore this mechanism by studying the structural properties of 23 spectroscopically identified recently quenched (or ‘post-starburst’ (PSB)) cluster galaxies at z ∼ 1. Despite clear PSB spectral signatures implying rapid and violent quenching, 87 per cent of these galaxies have symmetric, undisturbed morphologies in the stellar continuum. Remarkably, they follow a mass–size relation lying midway between the star-forming and quiescent field relations, with sizes 0.1 dex smaller than z ∼ 1 star-forming galaxies at log(M*/M⊙) = 10.5. This implies a rapid change in the light profile without directly effecting the stellar distribution, suggesting changes in the mass-to-light ratio gradients across the galaxy are responsible. We develop fading toy models to explore how star-forming galaxies move across the mass–size plane as their stellar populations fade to match those of the PSBs. ‘Outside-in’ fading has the potential to reproduce the contraction in size and increase in bulge-dominance observed between star-forming and PSB cluster galaxies. Since cluster PSBs lie on the large size end of the quiescent mass–size relation, and our previous work shows cluster galaxies are smaller than field galaxies, the sizes of quiescent galaxies must grow both from the quenching of star-forming galaxies and dry minor mergers.

scholarly journals Superdense massive galaxies in the nearby universe

2009 ◽  
Vol 5 (S262) ◽  
pp. 331-332
Author(s):  
Anna Ferré-Mateu ◽  
Ignacio Trujillo
Keyword(s):  
Value Added ◽  
Stellar Populations ◽  
Stellar Mass ◽  
Local Universe ◽  
Massive Galaxies ◽  
The Past ◽  
Mass Size ◽  
Size Relation

AbstractAt high-z the most superdense massive galaxies are supposed to be the result of gas-rich mergers resulting in compact remnant (Khochfar & Silk (2006); Naab et al. (2007)). After this, dry mergers are expected to be the mechanism that moves these very massive galaxies towards the current stellar mass size relation. Whitin these merging scenarios, a non-negligible fraction (1-10%) of these galaxies is expected to survive since that epoch retaining their compactness and presenting old stellar populations in the past universe.Using the NYU Value-Added Galaxy Catalog (DR6), we find only a tiny fraction of galaxies (~0.03%) with re ≤ 1.5 kpc and M* ≥ 8x1010M⊙ in the local Universe (z~0.2). Surprisingly, they are relatively young (~2Gyr) and metal rich ([Z/H]~0.2) These results have been published in Trujillo et al. (2009)

scholarly journals The environmental dependence of the stellar-mass-size relation in STAGES galaxies

2009 ◽  
Vol 402 (1) ◽  
pp. 282-294 ◽  
Author(s):  
David T. Maltby ◽  
Alfonso Aragón-Salamanca ◽  
Meghan E. Gray ◽  
Marco Barden ◽  
Boris Häußler ◽  
...  
Keyword(s):  
Stellar Mass ◽  
Mass Size ◽  
Size Relation ◽  
Environmental Dependence

scholarly journals Understanding the size growth of massive galaxies through stellar populations

2015 ◽  
Vol 11 (S319) ◽  
pp. 114-117
Author(s):  
I. Ferreras ◽  
I. Trujillo ◽  
E. Mármol-Queraltó ◽  
P. Pérez-González ◽  
Keyword(s):  
Stellar Populations ◽  
Stellar Mass ◽  
Massive Galaxies ◽  
Significant Process ◽  
Size Growth ◽  
Minor Mergers ◽  
Mass Increase ◽  
Massive Galaxy ◽  
Main Growth

AbstractMassive early-type galaxies undergo a significant process of evolution with redshift on the stellar mass vs size plane. Furthermore, this trend does not depend on the age of their stellar populations. Therefore, such an evolution should involve processes that do not include a significant amount of star formation, leaving (mostly) dry mergers as the main growth channel. By studying close pairs involving a massive galaxy, one can quantify the role of mergers on the growth of massive galaxies. A recent study based on the SHARDS dataset reveals that minor mergers cannot be the dominant mechanism to explain the bulk of size growth in these systems. Merging is found to provide a constant fractional growth rate of ~10% per Gyr from redshift z=1, corresponding to an overall stellar mass increase of 2× between z=1 and z=0.

scholarly journals A universal stellar mass-size relation of galaxies in the GOODS-North region

2012 ◽  
Vol 422 (2) ◽  
pp. 1014-1027 ◽  
Author(s):  
Takashi Ichikawa ◽  
Masaru Kajisawa ◽  
Mohammad Akhlaghi
Keyword(s):  
Stellar Mass ◽  
Mass Size ◽  
Size Relation

scholarly journals The stellar mass–size relation for the most isolated galaxies in the local Universe★

2013 ◽  
Vol 434 (1) ◽  
pp. 325-335 ◽  
Author(s):  
M. Fernández Lorenzo ◽  
J. Sulentic ◽  
L. Verdes-Montenegro ◽  
M. Argudo-Fernández
Keyword(s):  
Stellar Mass ◽  
Local Universe ◽  
Isolated Galaxies ◽  
Mass Size ◽  
Size Relation

scholarly journals Half-mass Radii for ∼7000 Galaxies at 1.0 ≤ z ≤ 2.5: Most of the Evolution in the Mass–Size Relation Is Due to Color Gradients

2019 ◽  
Vol 877 (2) ◽  
pp. 103 ◽  
Author(s):  
Katherine A. Suess ◽  
Mariska Kriek ◽  
Sedona H. Price ◽  
Guillermo Barro
Keyword(s):  
Mass Size ◽  
Color Gradients ◽  
Size Relation

scholarly journals SDSS-IV MaNGA: galaxy gas-phase metallicity gradients vary across the mass–size plane

2020 ◽  
Vol 501 (1) ◽  
pp. 948-953
Author(s):  
N F Boardman ◽  
G Zasowski ◽  
J A Newman ◽  
S F Sanchez ◽  
A Schaefer ◽  
...  
Keyword(s):  
Gas Phase ◽  
Physical Interpretation ◽  
Stellar Mass ◽  
Instrumental Effects ◽  
Physical Origin ◽  
The Galaxy ◽  
Mass Size ◽  
Nearby Galaxies

ABSTRACT Gas-phase abundances and abundance gradients provide much information on past stellar generations, and are powerful probes of how galaxies evolve. Gas abundance gradients in galaxies have been studied as functions of galaxies’ mass and size individually, but have largely not been considered across the galaxy mass–size plane. Thus, we investigate gas-phase abundance gradients across this plane, using a sample of over 1000 galaxies selected from the MApping Nearby Galaxies at APO (MaNGA) spectroscopic survey. We find that gradients vary systematically such that above 1010 M⊙, smaller galaxies display flatter gradients than larger galaxies at a given stellar mass. This mass–size behaviour cannot be explained by instrumental effects, nor is it simply a reflection of known trends between gradients and morphology. We explore multiple possibilities for a physical origin for this pattern, though further work is needed to establish a firm physical interpretation.

Advantages and limitations on combining radar dual - wavelength and polarimetric observations for ice microphysics retrievals

2021 ◽  
Author(s):  
Eleni Tetoni ◽  
Florian Ewald ◽  
Gregor Möller ◽  
Martin Hagen ◽  
Tobias Zinner ◽  
...  
Keyword(s):  
Dual Wavelength ◽  
Shape Estimation ◽  
Radar Observations ◽  
Microphysical Properties ◽  
Aspect Ratios ◽  
Retrieval Scheme ◽  
Mass Size ◽  
Ice Microphysics ◽  
German Aerospace ◽  
Size Relation

<p>The challenge of the ice microphysical processes representation in numerical weather models is a well-known phenomenon as it can lead to high uncertainty due to the variety of ice microphysics. As ice microphysical properties can strongly affect the initiation of precipitation as well as the type and amount of it, we need to better understand the complexity of ice processes. To accomplish this, better microphysics information through ice retrievals from measurements is needed. The multi-wavelength radar method is nowadays becoming more and more popular in such microphysics retrievals. Taking advantage of different scattering regimes (Rayleigh or Mie), information about the size of atmospheric hydrometeors can be inferred using different radar bands. For this study, dual-wavelength reflectivity ratio measurements were combined with polarimetric measurements to estimate the size of ice hydrometeors. The measurements were obtained by using the synergy of the C-band POLDIRAD weather radar from the German Aerospace Center, located in Oberpfaffenhofen, and the Ka-band MIRA-35 cloud radar from the Ludwig Maximilian University of Munich. Along with the dual-wavelength dataset, the Differential Reflectivity (Z<sub>DR</sub>) from POLDIRAD was used as a polarimetric contribution for the shape estimation of the detected ice particles. The radar observations were compared with T-matrix scattering simulations for the development of a retrieval scheme of ice microphysics. In the course of these studies, different assumptions were considered in the simulations. To capture the size variability, a Gamma particle size distribution (PSD) with different values of median volume diameter (MVD) was used. The soft spheroid approximation was used to approximate the ice particle shapes and to simplify the calculation and variation of their aspect ratios and effective densities. The selection of the most representative mass-size relation was the most crucial for the scattering simulations. In this study, we explored the modified Brown and Francis as well as the aggregates mass-size relation. After comparing the simulations to radar observations, we selected the better fitting one, i.e. aggregates, excluding the Brown and Francis as the simulated particles appeared to be too fluffy. Using the aggregates formulas, Look-Up tables (LUTs) for MVD, aspect ratio, and IWC were developed and used in the ice microphysics retrieval scheme. Here, we present preliminary microphysics retrievals of the median size, shape, and IWC of the detected hydrometeors combining the simulations in LUTs with the radar observations from different precipitation events over the Munich area.</p>

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